Starburst Galaxies Star Formation History of the Universe . There are a few cases where galaxies have been identified as Type II only because the broad components of the spectral lines have been very hard to detect. This seems to create nearly perfect conditions for generating diffuse … 1998), whereas radio-quiet quasars have q values lying in a similar range to local starburst galaxies and ULIRGs (Sopp & Alexander 1991). Red giant High mass star Low mass star Diffuse cloud Embedded protostar Molecular cloud Gravitational collapse Gravitational collapse Gravitational collapse Stellar wind Supernova explosion Stellar wind, UV radiation Dense clumps. The observations suggest quasars may starve this type of galaxy of energy needed to form stars. We present early X-ray results from Chandra for two starburst galaxies, M82 and NGC3256, obtained using ACIS-I and the HRC. For starburst galaxies and ULIRGs, q is observed to lie in the range 2.0 < q < 2.6 (Condon et al. Astrometry reveals that most of the X-ray sources are not coincident with the family of compact radio sources believed to be SNRs. Astronomers have located quasars inside four dusty starburst galaxies. Although Galactic cosmic rays (protons and nuclei) are widely believed to be dominantly accelerated by the winds and supernovae of massive stars, definitive evidence of this origin remains elusive nearly a century after their discovery [1]. Overview Motivation and historical approach The starting point: The physics and chemistry … Post-starburst galaxies can be identified via the presence of prominent Hydrogen Balmer absorption lines in their spectra. The search for TeV gamma-ray radiation from starburst galaxies (SBGs) has been conducted by the Whipple 10-m gamma-ray telescope from January 2001 to March 2003.

Overview.

We present a comprehensive study of the origin of strong Balmer lines in a volume-limited sample of 189 galaxies with 0.019.5 and projected axis ratio b/a>0.32. Cosmic rays are believed to be mainly accelerated by the winds and supernovae of massive stars, although definite evidence for this is lacking. 1991). For M82 the arcsecond spatial resolution enables us to separate the point source component from the extended emission for the first time.

The regions with high star formation rates (SFRs) observed in SBGs are frequently accompanied by high density clouds of interstellar mat-ter (ISM).

Roy et al. The origin of the differences between Type I and Type II Seyfert galaxies is not known yet. Radio-loud quasars, on the other hand, have typical q values in the range 0 < q < 1 (e.g.